日本地球惑星科学連合2019年大会

講演情報

[E] ポスター発表

セッション記号 A (大気水圏科学) » A-OS 海洋科学・海洋環境

[A-OS11] 陸域海洋相互作用-惑星スケール物質循環

2019年5月29日(水) 15:30 〜 17:00 ポスター会場 (幕張メッセ国際展示場 8ホール)

コンビーナ:山敷 庸亮(京都大学大学院総合生存学館)、升本 順夫(東京大学大学院理学系研究科)、Behera Swadhin(Climate Variation Predictability and Applicability Research Group, Application Laboratory, JAMSTEC, 3173-25 Showa-machi, Yokohama 236-0001)、佐々木 貴教(京都大学 大学院理学研究科 宇宙物理学教室)

[AOS11-P04] Numerical simulation of Tidal Heating using SPH and its application to inner sea formation

*村嶋 慶哉1山敷 庸亮1細野 七月2 (1.京都大学、2.海洋開発研究機構)

キーワード:氷衛星、潮汐加熱

There are some traces of liquid in icy moons, such as a plume of vapor of Europa acquired by Hubble Space Telescope and tiger stripes of Enceladus observed by Cassini. Since liquid water is essential for the origin of life, it can be important to understand the development of inner sea and also the temperature distribution inside of such icy moons.



It is considered that the tidal heating caused by tidal acceleration melts the inner icy layer which results in the presence of liquid water beneath its surface. Thus, we aim at simulating the tidal heating of an icy moon by 3-dimensional numerical fluid calculation in Smoothed Particle Hydrodynamics (SPH) method. As the tidal heating model, we apply the viscosity model which was used for numerical calculation of tidal stripping.



It is confirmed that this viscosity model lead to qualitatively correct result about tidal disruption, but the possibility of its application to tidal heating is not validiated. Therefore, as a first step, we tried to compare the result of this simulation with the result which is estimated theoretically. We made a rotation of a differentiated Titan-sized tidally locked object around a Saturn-mass material point with the radius of orbit being 1.1 times larger than its Roche limit. We also considered how to applicate this simulation to the calculation of actual icy moons. We will report the progress.